[22.06] Oxygen Chemistry in Titanís Atmosphere

Oxygen chemistry in the atmosphere of Titan is controlled by
the presence of CO and a likely influx of extraplanetary
oxygen. The presence of water vapor, corroborated by the
Infrared Space Observatory (ISO) stratospheric detection
[1], combined with CO induces the formation of CO2, which
has also been observed [2]. However, the high CO/H2O
ratio in Titan's atmosphere causes the propagation of oxygen
chemistry to follow a different path than what is predicted
for the Jovian planets. Specifically, the efficient CO
recycling mechanisms serve to inhibit significant formation
of larger oxygen compounds such as CH3OH (methanol) and
CH2CO (ketene). The results of a 1-D photochemical model
are presented in the context of identifying possible oxygen
compounds that might be detected by the Cassini/Huygens
mission which will arrive at Titan in 2004.

This work was supported by the NASA Planetary Atmospheres
Program and by the GCMS Project of the Cassini/Huygens
mission.